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Size Distributions of Solar Proton Events and Their Associated Soft X-Ray Flares: Application of the Maximum Likelihood Estimatorhttp://publi2-as.oma.be/record/4229
Cliver, E.W.Fri, 07 Jun 2019 13:48:35 GMThttp://publi2-as.oma.be/record/42292018Initiation of Stealth CMEs: Clues from Numerical Modelling and In-Situ Comparisonshttp://publi2-as.oma.be/record/4185
Talpeanu, Dana-Camelia Mon, 29 Apr 2019 13:26:57 GMThttp://publi2-as.oma.be/record/41852019Initiation of Stealth CMEs: Clues from Numerical Modelling and In-Situ Comparisonshttp://publi2-as.oma.be/record/4160
Talpeanu, Dana-CameliaThu, 07 Mar 2019 13:07:42 GMThttp://publi2-as.oma.be/record/41602018Numerical Modelling of Stealth Solar Eruptions Inserted in Different Solar Wind Speeds and Comparison with In-Situ Signatureshttp://publi2-as.oma.be/record/4159
Talpeanu, Dana-CameliaThu, 07 Mar 2019 12:48:03 GMThttp://publi2-as.oma.be/record/41592018SWAP Carrington Rotation Fileshttp://publi2-as.oma.be/record/4150
A Carrington Rotation is a period of time chosen to represent one rotation of the Sun, allowing the comparison of features such as sunspot groups or active regions. A period of 27.28 days was chosen to represent a single rotation that largely resembles the recurrence time of features near the equator. Each movie has a cadence of roughly 40 minutes, and each image is comprised of a median stacked set of smoothed SWAP images. By managing the images in this we're able to enhance the signal in the solar corona. The solar corona (the outer solar atmosphere) is seen as the ethereal region of the image surrounding the solar disk. During periods of high acitivty this region can be extremely dynamic showing complicated magnetic structures, as can be seen in the image below.West, MatthewMon, 11 Feb 2019 11:28:27 GMThttp://publi2-as.oma.be/record/41502018SWAP Carrington Rotation Fileshttp://publi2-as.oma.be/record/4149
A Carrington Rotation is a period of time chosen to represent one rotation of the Sun, allowing the comparison of features such as sunspot groups or active regions. A period of 27.28 days was chosen to represent a single rotation that largely resembles the recurrence time of features near the equator. Each movie has a cadence of roughly 40 minutes, and each image is comprised of a median stacked set of smoothed SWAP images. By managing the images in this we're able to enhance the signal in the solar corona. The solar corona (the outer solar atmosphere) is seen as the ethereal region of the image surrounding the solar disk. During periods of high acitivty this region can be extremely dynamic showing complicated magnetic structures, as can be seen in the image below.West, MatthewMon, 11 Feb 2019 11:28:23 GMThttp://publi2-as.oma.be/record/41492019SH33H-3727: Evolution of Coronal Cavity from Quiescent to Eruptive Phase in Association with Coronal Mass Ejectionhttp://publi2-as.oma.be/record/4010
The initiation mechanism of coronal mass ejections (CMEs) remains among the most elusive topics in solar physics. The initiation and triggering of CMEs can be studied by observing the coronal cavities in the lower coronal regions. These cavities appear as dark features and are believed to be the density depleted cross-sections of the magnetic flux ropes, where the magnetic field strength attains a much higher value compared to the background corona. Cavities may last for days or even weeks and evolve as the dark core part of the CME during the eruptive phase. In order to understand the pre-eruptive stability conditions for quiescent cavities and the triggering mechanisms for those structures to erupt, it is important to study the morphological evolution of the coronal cavities. In this work, we study the evolution of a cavity in lower corona using the observations from STEREO SECCHI/EUVI and PROBA2/SWAP EUV imager. In the quiescent phase, the cavity centroid height slowly rises from 1.10 to 1.23 RS during its passage on the visible solar disc from May 30 to June 13, 2010 and its initial circular shaped morphology gradually expanded and evolved into elliptical shape prior to the eruption from the western solar limb. The extended field-of-view of SWAP fills the observational gap between 1 to 2 RS . It enables us to capture the complete evolution of the erupting cavity starting from its EUV counterpart in the lower corona up to the white light cavity morphology seen in LASCO C2/C3 field-of-view. During the eruptive phase, we have observed a significant non-radial motion of the cavity at a very low coronal height of 1.3 RS . Furthermore, the geometrical fitting to the cavity morphology in different time-steps during its eruptive phase reveals that it exhibits non-self similar expansion in the lower corona. We also discuss the role of the background magnetic field and the possible instabilities which may lead to the non-radial motion and initiation of the cavity eruption respectively.Sarkar, RanadeepWed, 30 Jan 2019 22:01:52 GMThttp://publi2-as.oma.be/record/40102018Automated EUV Wave Catalogue For Solar Cycle 23 And 24: EUV Global Wave Rotation Sense Follows Hale Magnetic Cyclehttp://publi2-as.oma.be/record/3820
EUV global waves are among the best and earliest signatures of geoeffective Coronal Mass Ejections. In this work, we present the automatically constructed EUV global coronal waves (EIT waves) catalogue, a result of the application of the Novel EIT wave Machine Observing (NEMO) tool on the EUV solar images archives covering the intervals: 1997 March–2010 February (provided by EIT/SOHO telescope), January 2008 - December 2010 (provided by EUVI/SECCHI/STEREO) and January 2011 - December 2018 (provided by SWAP/PROBA2). Thus, we have studied the EUV waves characteristics through the evolution of the 23th and 24th solar cycle. The NEMO statistics show that small-scale EUV waves(mini-CMEs), firstly detected with SECCHI data, unambiguously contribute to solar wind formation in the outer corona. The possibility that the size and the intensity of eruptive dimming follow a power-law distribution could indicate that mini-CMEs observed in EUV solar corona are not different from the larger well defined EUV global waves. The amplitude-velocity ratio has been found to be also invariant for the statistically significant number of the propagating EUV waves fronts. It is demonstrated that the sense of EUV waves fronts rotation (clockwise or counter-clockwise) changes when initiated in different hemispheres (North or South). This sense of wave front rotation changes during solar maximum period, depending on the direction of the main magnetic sunspot of the active region (where event has been initiated) and follows Hale magnetic cycle. The consistent pattern of EUV waves rotation may contribute to the understanding of the future direction of the CME propagation.Podladchikova, OlenaWed, 23 Jan 2019 11:26:52 GMThttp://publi2-as.oma.be/record/382020193D Reconstruction and Simulation of Stealth CMEshttp://publi2-as.oma.be/record/3808
Mierla, MarilenaMon, 21 Jan 2019 16:26:55 GMThttp://publi2-as.oma.be/record/38082018Long-term evolution of the solar corona using SWAP datahttp://publi2-as.oma.be/record/3801
Mierla, MarilenaMon, 21 Jan 2019 16:10:02 GMThttp://publi2-as.oma.be/record/38012018Long-term evolution of the solar corona using SWAP datahttp://publi2-as.oma.be/record/3799
Mierla, MarilenaMon, 21 Jan 2019 16:07:21 GMThttp://publi2-as.oma.be/record/37992018Exceptional Extended Field of View Observations by SWAP on 1st and 3 April 2017http://publi2-as.oma.be/record/3666
On the 1st and 3rd April 2017 two large solar eruptions, which were associated with an M4.4 and an M5.8 class flare, respectively, were observed on the solar western limb with the Sun Watcher with Active Pixels and Image Processing (SWAP) EUV solar telescope on board the Project for On Board Autonomy 2 (PROBA2) spacecraft. The large field-of-view of SWAP, with the exceptional addition of the satellite being in a favorable off-pointed position to view the events, allow us to study the eruptions up to approximately 2 solar radii (${R}_{s}$), where space-based coronograph observations begin. SWAP observations reveal off-limb erupting features as well as on disk EUV waves initiated by these eruptions. Using this unique set of observations, the evolution of these two events is tracked and the propagating speeds of both the eruptions and the on-disk EUV waves are calculated.O'Hara, J.Tue, 18 Dec 2018 10:10:53 GMThttp://publi2-as.oma.be/record/36662018Exceptional Extended Field of View Observations by SWAP on 1 and 3 April 2017http://publi2-as.oma.be/record/3658
On the 1st and 3rd April 2017 two large solar eruptions, which were associated with an M4.4 and M5.8 class flare, respectively, were observed on the solar western limb with the PROBA2/SWAP telescope. The large field of view of SWAP combined with the exceptional circumstances of the satellite being off-pointed in a favorable position to view the events, provide us with the rare opportunity to study these eruptions up to approximately 2 solar radii, where space-based coronagraph observations begin. SWAP observations reveal off-limb erupting features as well as on disk EUV waves initiated by these eruptions. Using this unique set of observations, the evolution of these two events is tracked and the propagating speeds of both the eruptions and the on-disk EUV waves are calculated.O'Hara, JenniferTue, 27 Nov 2018 16:02:14 GMThttp://publi2-as.oma.be/record/36582018Exceptional Extended Field of View Observations by SWAP on 1 and 3 April 2017http://publi2-as.oma.be/record/3657
On the 1st and 3rd April 2017 two large solar eruptions, which were associated with an M4.4 and M5.8 class flare, respectively, were observed on the solar western limb with the PROBA2/SWAP telescope. The large field of view of SWAP combined with the exceptional circumstances of the satellite being off-pointed in a favorable position to view the events, provide us with the rare opportunity to study these eruptions up to approximately 2 solar radii, where space-based coronagraph observations begin. SWAP observations reveal off-limb erupting features as well as on disk EUV waves initiated by these eruptions. Using this unique set of observations, the evolution of these two events is tracked and the propagating speeds of both the eruptions and the on-disk EUV waves are calculated.O'Hara, JenniferTue, 27 Nov 2018 15:53:40 GMThttp://publi2-as.oma.be/record/36572018Numerical Modelling of Stealth Solar Eruptions and Comparison with In-Situ Signatures at 1AUhttp://publi2-as.oma.be/record/3619
Talpeanu, Dana-CameliaThu, 04 Oct 2018 14:38:09 GMThttp://publi2-as.oma.be/record/36192018Numerical Modelling of Stealth Solar Eruptions; Simulated and In-Situ Signatures at 1AUhttp://publi2-as.oma.be/record/3618
Talpeanu, Dana-CameliaThu, 04 Oct 2018 14:31:18 GMThttp://publi2-as.oma.be/record/36182018SWAP and LYRA onboard PROBA2http://publi2-as.oma.be/record/3571
D'Huys, ElkeWed, 19 Sep 2018 13:40:25 GMThttp://publi2-as.oma.be/record/35712018Ruimtevaarthttp://publi2-as.oma.be/record/3570
D'Huys, ElkeWed, 19 Sep 2018 13:31:44 GMThttp://publi2-as.oma.be/record/35702018De zon en ruimteweerhttp://publi2-as.oma.be/record/3569
D'Huys, ElkeWed, 19 Sep 2018 13:31:02 GMThttp://publi2-as.oma.be/record/35692018De Zon http://publi2-as.oma.be/record/3568
D'Huys, ElkeWed, 19 Sep 2018 13:30:15 GMThttp://publi2-as.oma.be/record/35682018Size distributions of solar proton events and their asso-ciated soft X-ray flares based on the maximum likelihood estimatorhttp://publi2-as.oma.be/record/3567
Cliver, E.W.Wed, 19 Sep 2018 13:20:07 GMThttp://publi2-as.oma.be/record/35672018THE SWAP EUV IMAGER ONBOARD PROBA2: 9 YEARS OF OBSERVATIONShttp://publi2-as.oma.be/record/3566
D'Huys, ElkeWed, 19 Sep 2018 13:09:56 GMThttp://publi2-as.oma.be/record/35662018Density Fluctuations in a Polar Coronal Holehttp://publi2-as.oma.be/record/3565
Hahn, MichaelWed, 19 Sep 2018 13:06:04 GMThttp://publi2-as.oma.be/record/35652018Density Fluctuations in a Polar Coronal Holehttp://publi2-as.oma.be/record/3562
Hahn, MichaelWed, 19 Sep 2018 12:30:56 GMThttp://publi2-as.oma.be/record/35622018Brightening and Darkening of the Extended Solar Corona during the Superflares of September 2017http://publi2-as.oma.be/record/3529
Goryaev, Farid F. Thu, 05 Apr 2018 09:42:53 GMThttp://publi2-as.oma.be/record/35292018